Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...254..305a&link_type=abstract
Astronomy and Astrophysics, Vol.254, NO. FEB(I), P. 305, 1992
Astronomy and Astrophysics
Astrophysics
47
Wolf-Rayet Stars, Mass Loss, H I Line Emission, Interstellar Medium: Shells, Supernovae And Supernovae Remnants
Scientific paper
The neutral hydrogen distribution has been studied in the direction of six galactic Wolf-Rayet stars using the 100-m Effelsberg radiotelescope. Neutral hydrogen deficiencies are observed to be associated with the Wolf-Rayet stars WR 3, WR 4, WR 5, WR 123, WR 132 and WR 140. These H I observations with intermediate angular resolution (9') show that the cavities are elongated structures having a mean axial ratio of the order of ˜2.2. Though H 1 maxima are always observed at the hole's periphery, they cover ≦ 80% of the H I void's boundary. The Wolf-Rayet stars are always off center with respect to either the geometrical center of the H I void or the absolute H I minimum inside the H I deficiency. On the average, they are offset by ˜50% of the H I hole's minor axis.
If Wolf-Rayet stars were progenitors of supernova explosions of type Ib, "barrel-shape" remnants may develop as a consequence of the matter distribution in the interstellar medium close to the Wolf-Rayet stars. The age of supernova remnants expanding within a previously evacuated cavity will be overestimated by a factor of roughly 4.4, when the standard model (non-wind, uniform density) of supernova remnant evolution is applied.
Due to the presence of holes in the matter distribution around WR stars, it is suggested that very young supernova remnants (age ≦500 yr?) formed by exploding WR stars may not be detectable by their characteristic radio continuum emission.
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